1 / 17

Superdense stars containing strange quark matter Yu.L.Vartanyan, A. R. Harutyunyan

Superdense stars containing strange quark matter Yu.L.Vartanyan, A. R. Harutyunyan. Yerevan State University. Strange quark matter.

morgan-hogan
Télécharger la présentation

Superdense stars containing strange quark matter Yu.L.Vartanyan, A. R. Harutyunyan

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Superdense stars containing strange quark matter Yu.L.Vartanyan, A. R. Harutyunyan Yerevan State University

  2. Strange quark matter In pioneer work of V.A.Ambartsumian and G.S. Sahakian [1] it has been shown that degenerated nuclear plasma may contain, besides neutrons, protons and electrons, also strange baryons – hyperons. In [2] G.S. Sahakian and Yu.L.Vartanian for the first time have shown that taking into account the interaction between baryons makes possible the existence of hyperons in the central regions of stable neutron stars. A new interest towards strange nuclear plasma has arisen when Witten [3] supposed, that quark-electron plasma with a strangeness -1 per baryon may be absolutely stable state of cold superdense matter. V.A.Ambartsumian, G.S. Sahakian, Sov.Astron.Zh.,37, 193,1960. G.S.Sahakian, Yu.L.Vartanian, Nuovo Cimento, 30, 82, 1963; Sov.Astron.Zh., 41, 193, 1964. E.Witten, Phys.Rev.D30, 272, 1984.

  3. Strange Stars Yu.L.Vartanyan, A.R.Arutyunyan, A.K.Grigoryan, Astrofizika, 37, 499,1994 (Astrophysics, 37, 271, 1994); Yu.L.Vartanyan, A.R.Arutyunyan, A.K.Grigoryan, Astronomy Letters, 21, 122, 1995.

  4. 90 1.4 70 1.1 50 E (MeV) 30 10 -10 -30 -50 0 0.2 0.4 0.6 0.8 n (fm-3) EoS for Strange Stars

  5. 15 7 10 1.1 R (km) 5 0 0 2 4 6 8 10 Radius-central density (SS)

  6. 2.5 7 2 1.1 1.5 M / MŸ 1 0.5 0 0 5 10 15 R (km) Mass-radius relationship (SS)

  7. r (km) Total energy density-distance from star center:1. M=0.5Msun, 2. M=1.44Msun, 3. M=1.86Msun

  8. EoS for Neutron Stars with a Strange Quark Core

  9. Neutron Stars with a Strange Quark Core Yu.L.Vartanian, A.R.Harutyunian, G.B.Alaverdyan, in the Plenary Lectures and Contributed Papers, GR 15, Pune, India, December 16-21, 1997, p.159; G.B.Alaverdyan, A.R.Harutyunyan, Yu.L.Vartanyan, Spacetime and Substance, 2, 3(8), 129, 2000; G.B.Alaverdyan, A.R.Harutyunyan, Yu.L.Vartanyan, Astrophysics, 44, 265, 2001; G.B.Alaverdyan, A.R.Arutyunyan, Yu.L.Vartanyan, Astronomy Letters, 28, 24, 2002; A.R.Harutyunyan, Astrophysics, 45, 248, 2002; G.B.Alaverdyan, A.R.Harutyunyan, Yu.L.Vartanyan, Astrofizika, 46, 445, 2003.

  10. First-order phase transition

  11. EoS for NS with a quark core

More Related